HUBBLE SPACE TELESCOPE<br /><br />DAILY REPORT # 3150<br /><br />PERIOD COVERED: DOY 183<br /><br />OBSERVATIONS SCHEDULED (see HSTARS below for possible observation problems)<br /><br />NICMOS 8790<br /><br />NICMOS Post-SAA calibration - CR Persistence Part 1.<br /><br />A new procedure proposed to alleviate the CR-persistence problem of NICMOS. Dark<br />frames will be obtained immediately upon exiting the SAA contour 23, and every<br />time a NICMOS exposure is scheduled within 50 minutes of coming out of the SAA.<br />The darks will be obtained in parallel in all three NICMOS Cameras. The POST-SAA<br />darks will be non-standard reference files available to users with a USEAFTER<br />date/time mark.<br /><br />STIS/CCD 8902<br /><br />Dark Monitor-Part 2.<br /><br />The Space Telescope Imaging Spectrograph (CCD) was used to monitor the darks.<br /><br />STIS/CCD 8904<br /><br />Bias Monitor-Part 2.<br /><br />The Space Telescope Imaging Spectrograph (CCD) was used to monitor the bias in<br />the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1 at gain = 4 in order<br />to build up high-S/N superbiases and track the evolution of hot columns.<br /><br />STIS/CCD 8905<br /><br />Read Noise Monitor.<br /><br />{A, B, C, D} on the STIS CCD using pairs of bias frames. Full frame and binned<br />observations are made in both Gain 1 and Gain 4, with binning factors of 1x1,<br />1x2, 2x1 and 2x2. All exposures are internals.<br /><br />STIS/MA1/MA2 8920<br /><br />Cycle 10 MAMA Dark Measurements.<br /><br />The Space Telescope Imaging Spectrograph (MA1 and MA2) was used to perform the<br />routine monitoring of the MAMA detector dark noise, and is the primary means of<br />checking on health of the MAMA detectors systems through frequent monitoring of<br />the background count rate.<br /><br />WF/PC-2 8935<br /><br />Cycle 10 Standard Darks.<br /><br />calibration of the CCD dark current rate, and to monitor and characterize the<br />evolution of hot pixels. Over an extended period these data will also provide a<br />monitor of radiation damage to the CCDs.<br /><br />WFPC2 8938<br /><br />WFPC2 CYCLE 9 SUPPLEMENTAL DARKS pt3/3.<br /><br />This dark calibration program obtains 3 dark frames every day to provide data<br />for monitoring and characterizing the evolution of hot pixels.<br /><br />WF/PC-2 8939<br /><br />Cycle 10 Internal Monitor.<br /><br />The WF/PC-2 was used to calibrate the internal monitor, to be run weekly to<br />monitor the health of the cameras.<br /><br />STIS/CCD 9066<br /><br />Closing in on the Hydrogen Reionization Edge of the Universe.<br /><br />The Space Telescope Imaging Spectrograph (CCD) was used in parallel constrain<br />the Hydrogen reionization edge in emission that marks the transition from a<br />neutral to a fully ionized IGM at a predicted redshifts.<br /><br />NICMOS 9269<br /><br />NICMOS Parallel Thermal Background<br /><br />NICMOS Camera 3 pure parallel exposures in the F222M filter will be obtained for<br />the entire duration of SMOV to establish the stability of the HST+NCS+Instrument<br />thermal emission.<br /><br />STIS/CCD 9317<br /><br />Pure Parallel Imaging Program: Cycle 10.<br /><br />The Space Telescope Imaging Spectrograph (CCD) was used to perform the default<br />archival pure parallel program for STIS during cycle 10.<br /><br />WF/PC-2 9318<br /><br />POMS Test Proposal: WFII Parallel Archive Proposal Continuation.<br /><br />The WF/PC-2 was used to perform the generic target version of the WFPC2 Archival<br />Pure Parallel program. The program was used to take parallel images of random<br />areas of the sky, following the recommendations of the Parallels Working Group.<br /><br />SNAP 9356<br /><br />SNAPSHOT survey of the Planetary Nebulae population of the Galactic Bulge<br /><br />The spectacular structures seen in HST images of planetary nebulae {PNe} are<br />generally accepted as originating from hydrodynamical interactions between<br />stellar winds: the interacting-stellar wind model {ISW}. Traditionally, the<br />shaping is thought to occur after the star becomes hot enough to ionize the PN.<br />But recent HST images indicate that the shaping may occur earlier, and the newer<br />GISW model puts the shaping during the pre-planetary nebula evolution. The<br />relative importance of both models is not known: GISW shaping will account for<br />some fraction of PNe, but estimates range from 15--100 during the PN phase,<br />especially for the youngest PNe. We here propose an HST SNAPshot survey of<br />compact PNe in the Galactic Bulge, to test these predictions. The Bulge provides<br />the only PNe population for which progenitor masses are known and nebular ages<br />can be measured. In support of these HST measurements we have already measured<br />velocity fields and emission line fluxes. The survey will give an unbiased<br />sampling of morphologies, and allow evolutionary sequences to be determined to<br />test the ISW versus the GISW model. By-products of the survey will be the<br />determination of nebular masses, diameters and filling factors. We will also<br />obtain the White Dwarf mass distribution in the Bulge, and the initial-final<br />mass function for low-mass stars.<br /><br />ACS 9363<br /><br />Ultra Low Surface Brightness Galaxies<br /><br />Extremely low surface brightness galaxies have been detected in the Virgo<br />cluster, which are 2 magnitudes fainter than any previously known in that<br />cluster or even in the Local Group. ACS images of three of these should resolve<br />stars at the giant branch tip, and allow us to determine distances, mean metal<br />abundance of the stars, and rough ages. Confirmation of the nature of these<br />galaxies will provide evidence that dark matter halos are pervasive in the<br />universe, extending to galaxies with stellar densities 6 times lower than<br />currently known. These resolved stars would be the most distant yet observed<br />accurately by HST.<br /><br />ACS/HRC 9391<br /><br />High-Resolution Imaging of Pluto's Surface<br /><br />We will collect a series of observations with the ACS/HRC from which we will<br />derive a two-color global map of Pluto's surface. We will image Pluto at F435W<br />and F555W, wavelengths that have been extensively studied from the ground over<br />the past 50 years. The maps will provide albedos with accurate error<br />determinations down to 52 degrees South latitude. These observations will<br />provide a second epoch of HST mapping of the active surface of Pluto as it<br />continues to recede from the Sun and will provide an important context for other<br />detailed studies of Pluto.<br /><br />ACS/CAL 9558<br /><br />ACS weekly Test<br /><br />for any source of noise in ACS CCD detectors. This programme will be executed<br />once a day for the entire lifetime of ACS.<br /><br />CAL/WF2 9597<br /><br />Intflat Sweep, Visflat Sweep, and Filter Anomaly Check<br /><br />No abstract available.<br /><br />WFPC2 9599<br /><br />WFPC2 Cycle 11 UV Earth Flats<br /><br />Monitor flat field stability. This proposal obtains sequences of earth streak<br />flats to improve the quality of pipeline flat fields for the WFPC2 UV filter<br />set. These Earth flats will complement the UV earth flat data obtained during<br />cycles 8-10.<br /><br />STIS 9618<br /><br />STIS MAMA Dispersion Solutions<br /><br />Obtain wavecals just deep enough to constrain wavelength and spatial distortion<br />maps without overusing the calibration lamp. For the first time on orbit, data<br />will be obtained at all available central wavelengths. This information will<br />help constrain global models of STIS optical performance being developed at ECF<br />and STScI. During the observations, MSM monthly offsets will be set to zero to<br />complement observations over the past couple of cycles, which occurred at extreme<br />monthly offsets. The echelle observations at zero offset will yield dispersion<br />solutions that are directly applicable to all echelle science data obtained<br />after monthly offsets are disabled.<br /><br />FLIGHT OPERATIONS SUMMARY:<br /><br />HSTARS: (For details see http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf)<br /><br />HSTARS: None<br /><br />COMPLETED OPS REQs:<br />16795-0 NICMOS Rotation Matrix Update @ 183/1346z<br />16797-0 Genslew for proposal 9678- slot # 3 @ 183/2038z<br /><br />OPS NOTES EXECUTED: NONE<br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 8 8<br />FGS REacq 9 9<br />FHST Update 9 9<br />LOSS of LOCK None<br /><br />Operations Notes: CCS PSS Acceptance Testing scheduled 184/12:00Z - 16:00Z<br />with HITT, SOC, GDOC, and VISN DOC using CCS "C" String with CCS Release 3.5<br />and OPSPRD O06100R1T<br /><br />SIGNIFICANT EVENTS: None